2015A&A...583A.121K


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.07CEST00:52:00

2015A&A...583A.121K - Astronomy and Astrophysics, volume 583A, 121-121 (2015/11-1)

Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud.

KAVANAGH P.J., SASAKI M., BOZZETTO L.M., POINTS S.D., FILIPOVIC M.D., MAGGI P., HABERL F. and CRAWFORD E.J.

Abstract (from CDS):

We present a multi-frequency study of the supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud.We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio polarisation and magnetic field orientation, and performed an X-ray spectral analysis.We estimated the remnant's size to be 24.9(±1.5)x21.9(±1.5)pc, with the major axis rotated ∼29° east of north. Radio polarisation images at 3cm and 6cm indicate a higher degree of polarisation in the northwest and southeast tangentially oriented to the SNR shock front, indicative of an SNR compressing the magnetic field threading the interstellar medium. The X-ray spectrum is unusual as it requires a soft (∼0.2keV) collisional ionisation equilibrium thermal plasma of interstellar medium abundance, in addition to a harder component. Using our fit results and the Sedov dynamical model, we showed that the thermal emission is not consistent with a Sedov remnant. We suggested that the thermal X-rays can be explained by MCSNR J0512-6707 having initially evolved into a wind-blown cavity and is now interacting with the surrounding dense shell. The origin of the hard component remains unclear. We could not determine the supernova type from the X-ray spectrum. Indirect evidence for the type is found in the study of the local stellar population and star formation history in the literature, which suggests a core-collapse origin.MCSNR J0512-6707 likely resulted from the core-collapse of high mass progenitor which carved a low density cavity into its surrounding medium, with the soft X-rays resulting from the impact of the blast wave with the surrounding shell. The unusual hard X-ray component requires deeper and higher spatial resolution radio and X-ray observations to confirm its origin.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - Magellanic Clouds - X-rays: ISM

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9476 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5695 1
3 DEM L 97 HII 05 12 07.7 -67 06 54           ~ 8 0
4 [FHW95] LMC B0512-6710 SNR 05 12 28.0 -67 07 27           ~ 11 0
5 [WHO2011] A126 MoC 05 12 30 -67 09.2           ~ 2 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14871 1
7 ICRF J052930.0-724528 QSO 05 29 30.04217690 -72 45 28.5072742   19.61   17.895   ~ 79 1
8 SNR G327.4+00.4 SNR 15 48 20 -53 49.0           ~ 83 0
9 NAME LHB X 16 42.0 +02 19           ~ 260 0
10 ICRF J193925.0-634245 Sy2 19 39 25.02671 -63 42 45.6255   18.87 18.37 17.64   ~ 957 1
11 NAME Cyg Loop SNR 20 51.0 +30 40           ~ 824 0

    Equat.    Gal    SGal    Ecl

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2020.08.07-00:52:00

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